Prompt emission spectra from the photosphere of a GRB

By D. Giannios. 2006

135 citations recorded by the source corpus.

I explore the observational appearance of the photosphere of an ultrarelativistic flow with internal dissipation of energy ("dissipative" GRB model). As a case study, I use the magnetic reconnection model (AC model) that makes robust predictions on the energy dissipation rates at different radii in the flow. With analytical and numerical tools for the radiative transfer problem, I show that the flow develops a hot photosphere where inverse Compton scattering leads to highly non-thermal spectrum. For a wide range of luminosities and baryon loadings of the flow, this spectrum is very close to the observed prompt GRB emission. Its luminosity ranges from ∼3 to 20% of that of the total energy input.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/ef04487d085f6564b59a2780a0948950e615171e

How researchers see this paper

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In Astronomy and Astrophysics

1. Bing Zhang
2. B. Metzger
3. E. Quataert
4. D. Giannios
5. T. Thompson
6. A. Pe’er
7. N. Bucciantini
8. Pawan Kumar

In Nuclear and High Energy Physics

1. B. Metzger
2. D. Giannios
3. Bing Zhang
4. E. Quataert
5. J. McKinney
6. M. Petropoulou
7. N. Bucciantini
8. L. Sironi

Citations in the corpus

• The Proto-Magnetar Model for Gamma-Ray Bursts (2010, methodology): “We follow the model of Giannios (2006, 2008), who assumes that the dissipated energy heats the plasma smoothly throughout the flow (slow heating model; see Ghisellini & Celotti 1999; Stern & Poutanen 2004).”
• A New Method of Determining the Initial Size and Lorentz Factor of Gamma-Ray Burst Fireballs Using a Thermal Emission Component (2007, background): “Giannios 2006) or external shocks (Mészáros & Rees 1993; Dermer & Mitman 1999)) is yet uncertain, and can in principle occur at various locations.”
• Relativistic Jets Shine through Shocks or Magnetic Reconnection (2015, background): “4 Note however that the GRB prompt signature can be the result of photospheric emission from thermal electrons (Ghisellini& Celotti 1999; Giannios 2006; Pe’er et al. 2006). c© 2013 RAS, MNRAS000, 1–?? radiative efficiency f & 0.1 and by (ii) extended non-thermal distributions of the radiating…”
• Prompt GRB emission from gradual energy dissipation (2007, methodology): “In previous works (Giannios 2006; Giannios & Spruit 2007; hereafter G06 and GS07 respectively), we studied the radiative transfer close to the Thomson photosphere of the flow in the context of the magnetic reconnection model.”
• A Reconnection Switch to Trigger gamma-Ray Burst Jet Dissipation (2010, background): “…scatters may be required to thermalize the photons, and incomplete thermalization might lead to lower temperatures allowing up to γ ∼ 1000 while still obtaining consistency with the observed peak energy (Thompson 1994; Giannios & Spruit 2005; Giannios 2006; Giannios & Spruit 2007; Giannios 2008).”